Showing papers by "Charles H. Townes published in 1982"
TL;DR: In this article, it was shown that the best model to fulfill these requirements involves cloud generation through disruption of red giants by stellar collisions, ionization by a population of stars which is affected either by enhanced metal abundances or the death of the most massive stars, and gas disposal by star formation.
Abstract: Observations of infrared fine-structure line emission from compact clouds of ionized gas in the galactic center have been reported by Lacy et al (1979, 1980). These observations suggest the existence of a central black hole of nearly 3,000,000 solar masses and require mechanisms to generate, ionize, and dispose of the gas clouds. It is found that the best model to fulfill these requirements involves cloud generation through disruption of red giants by stellar collisions, ionization by a population of stars which is affected either by enhanced metal abundances or the death of the most massive stars, and gas disposal by star formation. Although the existence of a massive black hole cannot be ruled out, it would play no necessary role in this model and may cause the tidal disruption of stars at a rate such that their accretion into the black hole would produce more radiation than is observed.
275 citations
TL;DR: The pure rotational S(2) line of molecular hydrogen at 12.28 microns was looked for in 44 positions in the Orion moleular cloud with 6 in. beams and 35 km/s spectral resolution; it was detected in 27 positions as mentioned in this paper.
Abstract: The pure rotational S(2) line of molecular hydrogen at 12.28 microns was looked for in 44 positions in the Orion moleular cloud with 6 in. beams and 35 km/s spectral resolution; it was detected in 27 positions. Emission was observed over a velocity range of + or - 100 km/s. The lines are approximately symmetric, and have full widths at half maximum ranging from 100 km/s down to the resolution limit. The distribution of intensities and line shapes is largely consistent with that seen in the 2 micron hydrogen transitions. However, unexpectedly complex line profiles and point-to-point variations in linear shapes appear, particularly in the region near IRc9.
9 citations
Journal Article•
TL;DR: In this article, the authors detecte les raies de structure fine [OI] 63,2 μm and [OIII]88,4 μm dans un faisceau de 44″ en direction du noyau de la galaxie M82.
Abstract: On a detecte les raies de structure fine [OI] 63,2 μm et [OIII]88,4 μm dans un faisceau de 44″ en direction du noyau de la galaxie M82. Chaque raie a un flux total de 2×10 −17 Wcm −2 . On evalue l'abondance de O ++ , O ++ /O=0,20 pour les regions HII dans le noyau. Il semble probable que la raie [OI] dans l'IR lointain provienne d'un objet compact situe loin du centre de M82, ou d'un nuage de poussiere intergalactique a travers lequel M82 se deplace